Spectroscopy helium atmosphere

Details of the experimental procedure used in scanning electron microscope CSEM ) and photoelectron spectroscopy CXPS> stre described in 133. The pore structure was determined with a Carlo Erba 2000 porosimeter. The thermogravimetric unalysis was carried out with the help of a Paulik-Paulik-Erdey Q-1500 D derivatograph in the helium atmosphere. 

We know today that hydrogen and helium are overwhelmingly the most abundant species in the atmospheres of the outer planets, but direct evidence for their presence was virtually absent prior to the work mentioned [145]. Supermolecular spectroscopy had to be discovered before such evidence could be understood and it comes as no surprise that soon after Welsh s discovery many other uses of collision-induced absorption were pointed out in various astrophysical studies. Supermolecular absorption and emission have become the spectroscopy of the neutral, dense regions, especially where non-polar gases prevail. 

ASTROCHEMISTRY. Application of radioastronomy (microwave spectroscopy) to determination of the existence of chemical entities in the gas clouds of interstellar space and of elements and compounds in celestial bodies, including their atmospheres. Such data aie obtained from spectrographic study of the light from the sun and stars, from analysis of meteorites, and from actual samples from the moon. Hydrogen is by far the most abundant element in interstellar space, with helium a distant second. 

The reaction of non-oxidizing dehydrogenation of n-hexane was carried out in a flow quartz reactor with a stationary layer of catalyst at atmospheric pressure in a stream of high purity helium. The optimum conditions of the reaction have been found by variation of volume velocity from 2.4 to 12 h and temperature in the range 500-700 C. Reaction products were analyzed by chromatography (Chrom-5), chromatomasspectroscopy (MX 1331) and IR-spectroscopy (Specord) methods. 

The development of many alternative plasma sources has led to a resurgence of analytical atomic emission spectroscopy in recent years. The major plasma emission sources used for gas chromatographic detection have been the microwave-induced helium plasma, under atmospheric or reduced pressure (MIP), and the DC argon plasma (DCP). The inductively coupled argon plasma (ICP) has been used much less for GC than as an HPLC detector [4]. 

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