Nuclear reaction studies on unstable isotopes can strongly help in improving our understanding of nucleosynthesis in stars.Indirect approaches to determining astrophysical reaction rates are increasingly common-place ...Nuclear reaction studies on unstable isotopes can strongly help in improving our understanding of nucleosynthesis in stars.Indirect approaches to determining astrophysical reaction rates are increasingly common-place and undergoing continuous refinement.Of particular interest is the use of such indirect techniques at storage rings,which,among other aspects,allow to recycle rare unstable beams.We propose to investigate the reaction rates of astrophysical interest using indirect methods(surrogate,Trojan horse,etc.)in reverse kinematics at the IMP-CAS storage ring.Long lived radioactive ion beams,produced remotely,can be accelerated,and made to interact with light targets.The proposed reactions are^(85)Kr(p,p’γ),^(85)Kr(d,pγ),constraining the neutron flux in an s-process branching point,^(79)Se(p,p’γ),^(79)Se(d,pγ),constraining the temperature in s-process nucleosyntheses,and^(59)Fe(d,pγ),constraining core collapse supernovae.展开更多
文摘Nuclear reaction studies on unstable isotopes can strongly help in improving our understanding of nucleosynthesis in stars.Indirect approaches to determining astrophysical reaction rates are increasingly common-place and undergoing continuous refinement.Of particular interest is the use of such indirect techniques at storage rings,which,among other aspects,allow to recycle rare unstable beams.We propose to investigate the reaction rates of astrophysical interest using indirect methods(surrogate,Trojan horse,etc.)in reverse kinematics at the IMP-CAS storage ring.Long lived radioactive ion beams,produced remotely,can be accelerated,and made to interact with light targets.The proposed reactions are^(85)Kr(p,p’γ),^(85)Kr(d,pγ),constraining the neutron flux in an s-process branching point,^(79)Se(p,p’γ),^(79)Se(d,pγ),constraining the temperature in s-process nucleosyntheses,and^(59)Fe(d,pγ),constraining core collapse supernovae.
