In Section 2.1, we present the nonuniform dust distribution found by studying X-ray scattered halos.
However, some problems must be solved before the application of this analysis to the X-ray scattered halo.
Nearly all X-ray scattered halos are found by comparing the observed radial surface brightness with the point spread function (PSF) of the telescope used.
According to the results above, we conclude that the dust distribution in our galaxy can be probed with the help of X-ray scattered halos.
X-ray scattered data allows to follow the gradual polymerisation of silica on the surface of cylindrical micelles, giving the final product in less then 10 min.
In summary, because the scattering process is related to the properties of the dust grains, i.e. the space distribution, the chemical composition, and the radii of the dust grains, we can study those properties with the X-ray scattered halos.
Following the method of Lee and Ravel (2005) and Lee et al. (2009), the chemical composition of dust grain can also be estimated by studying X-ray scattered halos.
In the DXS measurements, the distribution of the X-ray scattered intensity (normalized to that of the referential un-implanted crystal) in the direction parallel to the reciprocal lattice vector qz (qz ~ Δϑ) is presented in Figure 4. Figure 4 Distributions of the DXS signal intensity for Cz-Si (a) and FZ-Si (b).
A novel multi-element Si-pad array operated in spectroscopic mode was designed in collaboration with Sintef to measure low-angle X-ray scattered photons in the energy range of 12 45 keV with an FWHM energy resolution of about 4 keV.
Some gamma rays scattered from one of RHESSI's nine detectors into an adjacent one.
The Bragg law was used to explain the interference pattern of X-rays scattered by crystals.
