Light nuclei are found in core-collapse supernova matter and in binary neutron star mergers. Their presence may impact the evolution of these systems by affecting the rate at which the weak reactions take place during the core collapse, or the dissolution of the remnant torus of accreted matter that is formed around the high-mass neutron star after a binary merger. Light nuclei could also influence the dissipative processes that determine the postmerger evolution and mass ejection from the remnant. Therefore, the study of light nuclei is essential to obtain a good description of these astrophysical events. In this work, we investigate the abundance of light nuclei that are produced in these stellar environments using a relativistic mean-field model in hot low-density matter. Since the temperatures reached in these events may go up to 50-100MeV, hyperons may also be present in these astrophysical environments and so there is a chance that light hypernuclei may also be found. Therefore in this work we analyze the abundances of light nuclei, hyperons and light hypernuclei in hot low-density stellar matter. The nuclear couplings that represent the interaction of these light nuclei with the medium need to be calibrated according to experimental data, which can be done using results from heavy-ion collisions. This calibration is currently being done using that from the INDRA collaboration (GANIL, Caen, France). Some preliminary results will also be discussed.
Organized by: Catarina Cosme