摘要
A kilonova is an optical-infrared transient powered by the radioactive decay of heavy nuclei from a binary neutron star merger.Its observational characteristics depend on the mass and the nuclide composition of merger ejecta,which are sensitive to the equation of state(EoS)of the neutron star.We use astrophysical conditions derived from different EoSs as nucleosynthesis inputs to explore the impact of various EoS on the r-process nucleosynthesis and the kilonova emission.Our results show that both the abundance patterns of merger ejecta and kilonova light curves are strongly dependent on the neutron star EoSs.Given the mass of two neutron stars,the merger with a softer EoS tends to generate a larger amount of ejected material,and may lead to a brighter kilonova peak luminosity.The relationship between the neutron star EoS and the peak luminosity provides a probe for constraining the properties of EoS in multi-messenger observations of neutron star mergers.
基金
supported by the National Natural Science Foundation of China(NSFC,grant Nos.12403043,12347172,and 12133003)
M.H.C.also acknowledges support from the China Postdoctoral Science Foundation(grant Nos.GZB20230029 and 2024M750057)
supported by the Guangxi Talent Program(Highland of Innovation Talents).
