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Historically,Ge has been considered to be a neutron-capture element. In thiscase, the r-process abundance of Ge is derived by subtracting the s-processabundance from the total abundance in the Solar system. However, the Geabundance of the metal-poor star HD 108317 is lower than that of the scaledresidual r-process abundance in the Solar system, about 1.2 dex. In this paper,based on a comparison of the Ge abundances of metal-poor stars and stellaryields, we find that the Ge abundances are not the result of the primary-likeyields in massive stars and come mainly from the r-process. Based on theobserved abundances of metal-poor stars, we derived the Ge abundances of theweak r-process and main r-process. The contributed percentage of theneutron-capture process to Ge in the Solar system is about 59 per cent, whichmeans that the contributed percentage of the Ge residual abundance in the Solarsystem is about 41 per cent. We find that the Ge residual abundance is producedas secondary-like yields in massive stars. This implies that the element Ge inthe Solar system is not produced solely by the neutron-capture process.

Is Germanium (Ge, Z=32) A Neutron-Capture Element?