7-radiation superheavy

Both A(3> and B(3> are longitudinally directed and are nonzero in the vacuum. Both A(3> and B(3> are phaseless, but propagate with the radiation [47-62] and with their (1) and (2) counterparts. The radiated vector potential A<3 does not give rise to a photon on the low-energy scale, because it has no phase with which to construct annihilation and creation operators. On the high-energy scale, there is a superheavy photon [44] present from electroweak theory with an SU(2)x SU(2) symmetry. The existence of such a superheavy photon has been inferred empirically [44], However, the radiated vector potential A<3) is not zero in 0(3) electrodynamics from first principles, which, as shown in this section, are supported empirically with precision. 

But even if the half-lives of superheavy nuclides would not exceed the 108y level, there was hope to discover them in Nature. Although now extinct, they may have left detectable traces such as fission tracks or fission products in certain samples. Another possible source could be the cosmic radiation impinging on Earth whose heavy component may be formed by r-process nucleosynthesis in our galaxy not longer than 107 y ago [33] and may, hence, contain superheavy nuclei with half-lives down to some 105 years. 

Objections against these findings were soon raised. The strongest peak attributed to element 126 could experimentally be accounted for [55] by a prompt y-ray from the (p,n) nuclear reaction with natural 140Ce, a major component of the monazite crystals. The weaker peaks were shown to stem from to K x-rays from traces of ordinary elements such as antimony and tellurium [56]. When a more specific technique for the excitation of x-ray spectra was applied to the inclusions, namely by monochromatic synchrotron radiation tuned to the x-ray absorption edges, the evidence for superheavy elements vanished [57,58]. Furthermore, attempts failed [59] to detect them in bulk monazites through isolation of an A>294 fraction with a mass... 

Hot-fusion reactions were employed in the discoveries of the elements beyond mendelevium as far as element 106, producing the first three members of the domain of superheavy elements. Higher transactinides have also been synthesized in these reactions. As before, the general trends with increasing atomic number were shorter half-lives and smaller production cross sections, a consequence of decreased survival probability in the evaporation process [132, 133]. The probability of decay from the nuclear ground state by spontaneous fission became significant in these elements. The techniques used in the experiments still included radiochemistry and off-line radiation counting [134]. As half-lives dropped below minutes into seconds it became more common to use direct techniques like transportation in gas jets to mechanisms like wheels and tapes (see Sect. 3.3 and Experimental Techniques ). Detection of new nuclides resulted from the detailed... 

Another class of search for experiments is the measurement of heavy element abundances in the cosmic radiation by exposure to particle track detectors— nuclear emulsions or plastic sheets—in balloon flights at high altitudes with analysis of the recorded tracks for atomic number and abundance. A survey [33] of all data obtained until 1970 showed one single event beyond Z 100. With the data collected in the Skylab space station, the limit became more stringent no superheavy nucleus in spite of the 204 recorded tracks with atomic number 74—87 [77]. A similar hmit was deduced [78] after exposure in a satelhte. In a study of cosmic-ray induced tracks in olivine crystals enclosed in iron-stone meteorites, which were exposed in space over millions of years, unusually long tracks were found and attributed to superheavy elements [79, 80]. However, this conclusion could not be maintained [81, 82] after calibration experiments of track dimensions with energetic beams delivered by accelerators. 

Sparks, C.J., Raman, S., Yakel, H.L., Gentry, R.V., Krause, M.O. Search with synchrotron radiation for superheavy elements in giant-halo inclusions. Phys. Rev. Lett. 38, 205-208... 

---