2014 In previous papers [1-3] we have reported experimental measurements of the relaxation rates of the k-multipole moments in the 4D level of sodium and the 3S-4D optical coherence. In the present paper we compare the experimental values with those obtained theoretically for different types of potentials. We show that the Van der Waals C6R -6 interaction is not sufficiently anisotropic to desc...

• Unique pore structure enables the dense packing of Xe inside pores. Both high sorption capacity and Xe/Kr selectivity are achieved. The highest storage density at ambient conditions. For adsorptive separation xenon/krypton mixture, it still remains a daunting challenge to target both adsorption in single adsorbent because their close size inert nature. Herein, we report an ultra-microporous a...

The effect of water ice formation temperature and rate of ice deposition on a cold plate on the amount of trapped argon (equivalent to CO), and the ratios of Ar/Kr/Xe trapped in the water ice were studied at 50, 27 and 22 K and at ice formation rates ranging over four orders of magnitude, from 10 1 to 10 5 m min . Contrary to our previous conclusions that cometary ices were formed at 50–60 K, w...

An Enskog-Landau kinetic equation for a many-component system of charged hard spheres is proposed. It has been obtained from the Liouville equation with modified boundary conditions by the method of nonequilibrium statistical operator. On the basis of this equation the normal solutions and transport coefficients such as bulk κ and shear η viscosities, thermal conductivity λ, mutual diffusion D ...

The rotational structure in the vibrational transitions from v50 to v51, 2, 3, 4 of HCl and HCl is studied in Xe, Kr, and Ar matrices with high spectral resolution. A consistent set of rotational constants Bv for the vibrational levels v50 to 4 is derived. B0 decreases with the tightness of the cage from 9.78 cm in Xe to 8.83 cm in Ar for HCl ~gas phase 10.44 cm!. The values for B0 to B4 decrea...

Introduction: Martian meteorite studies have provided information on the composition of noble gases and nitrogen in the atmosphere and interior of planet Mars [1]. Two interior components (Chass-S, Chass-E) in Chassigny [2,3]; a mixture of interior (Chass-S) and modern Mars atmosphere in Shergottites [4], elementally fractionated atmosphere in Nakhlites [5] and ancient Mars atmosphere in ALH840...