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White-line emission

Fig. 2. (a) (b) Transmission electron microscopy (TEM) images of as-grown VGCFs (broken portion) with the PCNT core exposed field emission-type scanning electron microscopy (FE-SEM) image of (c) as-grown and (d) heat-treated VGCFs (broken portion) at 2800°C with PCNT (white line) exposed [20],... [Pg.146]

In a recent paper Overn10 has also given wave-lengths for these same emission lines. His values, however, do not agree with ours even when corrected for the difference between the rock salt grating space used by him and the calcite grating space used by us. The discrepancy between his values and ours seems to increase as we go farther from the white line used as a reference line by him. [Pg.5]

Multilayer devices with lanthanide chelate complexes. In these complexes, efficient energy transfer from the singlet or triplet exciton on the ligand of the complex to the lanthanide atom at its center results in efficient, atomic-like line emission spectra from the latter. By adjusting the identity and concentration of the different lanthanide complex dopants, a line spectrum with white CIE coordinates was achieved.77... [Pg.19]

According to colorimetry, the coordinates of a color, which is produced by the mixture of two colors, can be found on the connecting line between the coordinates of the two colors in the CIE graph. A mixture of the m-LPPP and PPDB emission colors therefore can produce white-light emission near the equienergy white point (x = 1/3, y = 1/3) (see Fig. 8.21). [Pg.232]

The possibility of tuning the shades becomes apparent when a plot of the CIE coordinates [15] is made from the spectra in Fig. 2. The CIE plot in Fig. 3 marks the coordinates for white light emission, css at 200 °C and 230 °C. A straight line connects all the coordinates. Thus, by controlling the temperature and time of heating it is possible to fine tune the exact shade of white light. [Pg.551]

Solar spectrum as well as line emission spectra characteristic of a series of metals (all spectra in black and white rather than color). The lines (bands) of the pure metals are emission lines from each metal. The solar spectrum lines (top) are lines of darkness in the continuous rainbowlike solar spectrum. These Fraunhofer lines (only the most intense are shown) arise from absorption of solar light by the corresponding metal present in the solar photosphere. Fraunhofer lines labeled A, a, B are due to absorption by O2 in the Earth s atmosphere. [Pg.10]

Figure 7.7 The line spectra of several elements. A, The line spectrum of atomic hydrogen. B, Unlike the continuous spectrum of white light, emission spectra of elements, such as mercury and strontium, appear as characteristic series of colored lines. Figure 7.7 The line spectra of several elements. A, The line spectrum of atomic hydrogen. B, Unlike the continuous spectrum of white light, emission spectra of elements, such as mercury and strontium, appear as characteristic series of colored lines.
In absorption spectra, under the same conditions as for emission lines, changes of structure and shifts are observed for the main edges, white lines, XANES and EXAFS. They are widely exploited. Refer to [1 to 5, 9 to 20] and especially to several proceedings of EXAFS conferences (cited on p. 240). [Pg.242]

If we pass white light through a vapor composed of the atoms of an element, we see its absorption spectrum, a series of dark lines on an otherwise continuous spectrum (Fig 1.11). The absorption lines have the same frequencies as the lines in the emission spectrum and suggest that an atom can absorb radiation only of those same frequencies. Absorption spectra are used by astronomers to identify elements in the outer layers of stars. [Pg.131]

Spectra and numerical data to illustrate this point are presented in Figure 8 and Table III. The best rare earth blijie line emitter is Tm ", but its emission, as typified by ZnS Tm (18) emission, peaks at 475 nm, wavelength that poorly matches the z curve thus z is low and Tm emission contributes ineffectively to a white field. [Pg.187]


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See also in sourсe #XX -- [ Pg.151 , Pg.173 ]




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