Addition deuterium

Tile first iwo equations represent tlie fact that the D-D reaction can follow either of Iwo paths, producing tritium and one proton or helium-3 and one neutron, wirli equal probability. The products of the first two reactions form the fuel for the third and fourth reactions, and they are burned with additional deuterium. The net reaction consists of the conversion of six deuterium nuclei into two helium nuclei, two hydrogen nuclei, and two neutrons along with a net energy release of 43.1 MeV. The reaciion products—helium, hydrogen, and neutrons—are harmless as... 

The reaction occurs slowly at normal temperature, but other unsaturated aldehydes also reacted. When 4-hexenal-l-d was used, the deuterium was found to be distributed over both carbon atoms of the former ethylene molecule. In addition, deuterium was found in the recovered gaseous ethylene, whilst some of the 6-octen-3-one product was deuterium-free. These observations are readily explained by the mechanism given in Scheme 63, in which alkene insertion and hydride elimination are faster than the reductive elimination of the final product. 

An additional deuterium plasma treatment at 350 °C results in one additional IR absorption line at 2644.4 cm . The frequency ratio of the 3577.3 cm line and the line at 2644.4 cm is 1.35, which is close to the value expected for a harmonic oscillator consisting of a hydrogen atom bound to an oxygen atom (1.37). Based on this, we identify the 3577.3 cm line as a LVM of an 0-H bond. No extra lines appear in the spectra after H+D plasma treatment. This strongly indicates that the defect responsible for the 3577.3 cm line includes a single hydrogen atom. 

Accretion of icy cometary matter has been widely viewed as a plausible source for Earth s water. The D/H ratio in seawater, however, is substantially lower—by a factor of -2—than in the few comets where D/H has been measured (Laufer et al. 1999). A significant contribution of terrestrial water by comets would still be permitted if their high D/H ratio were appropriately lowered by accretion of additional, deuterium-poor materials. Suggested possibilities for low D/H carriers include rocky planetary accretional components (Laufer et al. 1999), or a high influx during the heavy bombardment epoch of interplanetary dust particles heavily loaded with implanted solar-wind hydrogen (Pavlov et al. 1999). 

Thus upon prolonged irradiation the initially formed 2-deuterio-4-phenylthiazole 51-2d transposes to 5-deuterio-3-phenylisothiazole 47-5d without additional deuterium incorporation [36]. 

---