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The classical collision cross-sections of a proton with an argon atom as well as the thermal transport coefficients and rate constant of the colliding $\text{H}^{+}-\text{Ar}$ system are evaluated at the kinetic temperature $T\in [100,10\,000]~(\text{K})$ by means of the asymptotically correct analytical potential constructed for the ground $X^{1}\unicode[STIX]{x1D6F4}^{+}$ state of the ArH+ cation from the highly accurate ab initio data available in the entire range of internuclear distances (Terashkevich et al., J. Quant. Spectrosc. Radiat. Transfer, vol. 234, 2019, pp. 139–146). The results can be useful to estimate thermodynamic, transport and kinetic properties of the Ar/H2 plasma in a wide temperature range.
Signal separation is a common task in cosmological data analysis. The basic problem is simple to state: a number of signals are mixed together in some manner, either known or unknown, to produce some observed data. The object of signal separation is to infer the underlying signals given the observations.
A large number of techniques have been developed to attack this problem. The approaches adopted depend most crucially on the assumptions made regarding the nature of the signals and how they are mixed. Often methods are split into two broad classes: so-called blind and non-blind methods. Non-blind methods can be applied in cases where we know how the signals were mixed. Conversely, blind methods assume no knowledge of how the signals were mixed, and rely on assumptions about the statistical properties of the signals to make the separation. There are some techniques that straddle the two classes, which we shall refer to as ‘semi-blind’ methods. They assume partial knowledge of how the signals are mixed, or that the mixing properties of some signals are known and those of others are not.
There is a large literature in the field of signal processing about signal separation, using Bayesian techniques or otherwise. For any cosmological signal separation problem, it is almost always the case that someone has already attempted to solve an analogous problem in the signal processing literature. Readers who encounter a problem of this type, which is not already addressed in the cosmological literature, are encouraged to look further afield for existing solutions.
We processed coarse-grained Ti and equal-channel angular pressing (ECAP) processed ultrafine-grained (UFG) Ti into 20-μm-thick Ti foils by cold rolling and intermediate annealing. The foils produced from rolling the UFG Ti exhibit a homogeneous nanostructure, while foils produced from rolling the coarse-grained Ti exhibit heterogeneous structures with a mixture of nanostructured regions and coarse-grained regions. The former foils also have higher strength and ductility and exhibit uniform deformation over a larger strain range at room temperature than the latter ones. This work demonstrated the advantage and viability of producing nanostructured Ti foil by rolling ECAP-processed UFG Ti stock.
The preliminary results of monitoring of simultaneous spectra of a sample of extragalactic sources are given. Eight sets of observations were done at the RATAN-600 radio telescope in 1995-1996 at six frequencies (0.96, 2.3, 3.9, 7.7, 11.2, and 22 GHz). The light curves as well as the variability parameters are given
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