Radiative neutron capture reaction rates for stellar nucleosynthesis

There is a high demand for nuclear data in multidisciplinary subject like nuclear astrophysics. The two areas of nuclear physics which are most clearly related to one another are stellar evolution and nucleosynthesis. The necessity for nuclear data for astrophysical applications puts experimental methods as well as reliability and predicative ability of current nuclear models to the test. Despite recent, considerable advances, there are still significant issues and mysteries. Only a few characteristics of nuclear astrophysics are covered in the current work which include \(^{52}\)Fe(n,\(\gamma \))\(^{53}\)Fe, \(^{53}\)Fe(n,\(\gamma \))\(^{54}\)Fe, \(^{54}\)Fe(n,\(\gamma \))\(^{55}\)Fe, \(^{55}\)Fe(n,\(\gamma \))\(^{56}\)Fe, \(^{56}\)Fe(n,\(\gamma \))\(^{57}\)Fe, \(^{57}\)Fe(n,\(\gamma \))\(^{58}\)Fe and \(^{58}\)Fe(n,\(\gamma \))\(^{59}\)Fe reactions which are important in stellar nucleosynthesis. The reaction rates are calculated using nuclear statistical model. These rates are subsequently fitted to polynomials of temperature T\(_9\) in order to facilitate calculations for stellar nucleosynthesis.