Rapid proton capture in neutron star surface

The rapid-proton-capture process is examined in light nuclei starting with 22Ne at the neutron star surface. The extreme-density situation prevalent in the neutron star surface requires that the Coulomb term in the equation of nuclear masses is modified. The rise in temperature which may be as high as 108 K and a few times 109 K also is generally due to infall of matter from the binary companion. The Coulomb correction in the nuclear masses affects the proton binding energy Qsub(p) in the nuclei. Continuous proton addition in the nuclei depends on the Qsub(p) value, which when falls below a certain value will not capture further protons unless the nucleus undergoes β+-decay, thus increasing the proton binding energy and making the nucleus capable of capturing protons again. The capture path so obtained will be crucially dependent on the Qsub(p) value. It has been considered the change in the nuclear masses due to this correction effect for the calculation of the proton capture path. Four capture paths have been considered for Qsub(p) = 0.001 MeV, 0.16 MeV, 0.011 MeV and 0.26 MeV. Low-mass nuclei at each z are formed in the process. They are normally proton rich and undergo β+-decay giving their stable products. It is expected that the stable products of the proton-capturing chain in the neutron star surface may be reflected in the composition of cosmic rays if it is subscribed to the view that neutron stars are the source of acceleration of cosmic rays. It is suggested that this rapid-proton-capture process in the neutron star surface may help in understanding some γ-ray burst events associated with the neutron star surface