Study of level structure on 26 Si for the astrophysical interest in 26 Al production

Abstract

A radio-isotope of 26g Al (where g is expressing the ground state) is known as a -ray emitter spreading in the Milky Way galaxy. Since the half-life is only 7.2 × 10 5 year this is the obvious evidence of ongoing nucleosynthesis in our galaxy. This isotope is also known as an origin of abundance-anomaly of 26 Mg observed in meteorites. Therefore, investigations of production rates for the 26g Al are quite important for the nucleosynthesis occurring in massive star, classical nova and super nova. Although, there is still some uncertainties in the nuclear structure of 26 Si which is located at the bypass sequence producing the isomeric state 26m Al (where m is expressing the metastable 1 st excited state). For the comprehensive understanding of the nuclear reaction rate to produce the 26g Al, we have done -ray spectroscopy to investigate the level structure for the 26 Si. We confirmed the presence of a recently proposed level located just above the proton threshold. Furthermore, as a result of the gamma-ray angular correlation measurements we could assign the spin of this level as 0 + .