Decay of superstrings in the early universe and origin of primordial heavy elements

An alternative to standard big-bang cosmology is a scenario (Tassie 1986, 1987) of the formation of the universe from a cascade of exploding pieces of superstring. This scenario explains the correlation between the mass and angular momentum of many different scales of astronomical objects (Brosche and Tassie 1989) from superclusters of galaxies to planets The resulting fragments of superstring from each explosion will in turn explode yielding eventually the smallest possible pieces of superstring. Since, according to superstring theory, quarks and gluons are the smallest pieces of superstring, the decay of large pieces gives rise to a quark-gluon plasma, which can condense not only to baryons but also to a very small amount of multi-baryons, i.e. quark matter or heavier nuclei. Although the majority of the hadronic phase consists of nucleons, this small amount of heavier nuclei could play an important part in the subsequent primordial nucleosynthesis. If the number abundance of these seed nuclei is of order of 10^-15, then the produced nuclear abundances of heavier (A ≥ 9) elements are largely enhanced from the standard model values and amount to the 1% level of those observed in the most metal deficient population II giants, which show possibly an upper limit of primordial nuclear abundances. The light element abundances for D, He and Li are essentially the same as those predicted from the standard model without seeds. In this paper we first discuss the scenario (Tassie 1986, 1987; Brosche and Tassie 1989) for the formation of astronomical objects from superstring and then show calculated results of primordial heavy element abundances (Kajino and Tassie 1992) as possible observational evidence for our scenario.