Carbon-12 Reaction Rate on a Neutron Star in a Common Envelope Binary System

In this thesis I calculate a new reaction rate for 12C formed via the resonant reaction pathway that leads to formation of 12C in an excited state known as the Hoyle State. This research was precipitated by the discovery that the radiative width (Γ_rad) was 34 percent higher than the previously accepted value[1]. This is considerably larger than the uncertainty on the previously accepted value. I then used a scaling factor to assess the impact a higher rate could have on nucleosynthesis models using NuGrid. The astrophysical environment simulated was for a neutron star in a common envelope binary system. The neutron star spirals towards the centre of a late stage red giant; which provides the helium rich environment and the extreme temperature and pressure that is perfect for explosive nucleosynthesis
to occur. A primary example of explosive nucleosynthesis is the triple alpha process investigated by this research. My results, having used a scaling factor that increased the triple alpha reaction rate by 30 percent in line with my results. This appears to cause a significant increase in the abundance of 12C, in some instances 3 times more 12C is present compared to simulations using the old reaction rate.
This is the first time this has been investigated in this astrophysical environment. My results clearly show that Nucleosynthesis models are significantly impacted by the higher reaction rate for Carbon-12.