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X-ray spectrometer RESIK has observed spectra in the four wavelength bands from 3.3 Å to 6.1 Å.
It measured for the first time in a systematic way solar soft X-ray spectra in the four wavelength channels from 3.3 Å to 6.1 Å.
The solar radiation has been assayed in four wavelength bands (UV-C, 170 280 nm, UV-B, 280 315 nm), UV-A (315 400 nm) and PAR (photosynthetic active radiation, 400 700 nm).
Chemical composition of alloys/metals was determined by a Cameca Camebax Micro electron microprobe (EPMA) equipped with four wavelength dispersive spectrometers and a Kevex Analyst 8000 energy dispersive detector.
Therefore, to select most appropriate wavelength, MOX was determined form the laboratory mixture at all the four wavelength and mean recovery and standard deviation were calculated and found to be 101 ± 2.45, 100.89 ±1.48 99.81 ± 2.68 and 100.67 ± 0.73 at 222.1, 248.2, 379.0 nm and 287.0 nm respectively.
Analyses were carried out on a Cameca sx50 electron microprobe equipped with four wavelength dispersive X-ray spectrometers (WDS) and an energy dispersive X-ray spectrometer (EDS) using standard microprobe imaging and microanalytical methods [15], [16].
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The electron probe used for quantitative micro-analysis is a Cameca SX50, equipped with four wavelength-dispersive spectrometers.
STEREO's telescopes are tuned to four wavelengths of extreme ultraviolet radiation selected to trace key aspects of solar activity such as flares, tsunamis and magnetic filaments.
The commonly admitted limit for PO algorithm is between three to four wavelengths [2].
For the design used, this length was predicted to be four wavelengths.
Figure 3b gives the corresponding trends of reflectance for the four wavelengths.
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