Our yields increase with the mass of the progenitor main - sequence stars . massive stars ( i . e . 18m < m < 50m ) is the primary sites of the neclearsynthesis of the r - process and can explain the galaxy chemical evolution . 3 . we present formula to calculat the r - process galactic chemical evolution of ba peak elements . this formula contains metallicity abundance and point out the relation of the ba peak elements and disscuss the effect of various mass supersnova . besides , our formula can be confirmed by a lot of observations 由此可以解釋以下觀測事實: ( l ) mg , eu均產(chǎn)生于snh星,但質(zhì)量范圍不同,在高質(zhì)量( > 20 ) eu的產(chǎn)量高, mg的產(chǎn)量(相對于太陽) ,導(dǎo)致暈星中eu / mg > 0 ,而產(chǎn)生mg的質(zhì)量范圍較大,致使在厚盤的晚期較小質(zhì)量超新星也開始對mg有貢獻,而這些星對eu的貢獻很小,致使在厚盤星中eu / mg < 0 ,在厚盤中eu / fe隨金屬豐度的升高而降低,仁mg / fe隨金屬豐度的升高而不變
The dissertatation consists of two sections . the first one mainly intrduce the chemical evolution model and observational constrain , and the second mainly intrduce the ncleosyhthesis of r - process and the chemical evolution of ba peak elements the formation and evolution of the galaxy has long been a basic and important branch and one of the most active frontiers in the fields of astrophysics 本文分二部分,第一部分重點介紹星系的化學演化模型和觀測約束,第二部分重點介紹r - process核合成和ba峰元素r - process的星系化學演化。
The r-process is a nucleosynthesis process, that occurs in core-collapse supernovae (see also supernova nucleosynthesis), and is responsible for the creation of approximately half of the neutron-rich atomic nuclei heavier than iron. The process entails a succession of rapid neutron captures (hence the name r-process) by heavy seed nuclei, typically 56Fe or other more neutron-rich heavy isotopes.