Studies On Cooling Properties Of Massive Neutron Stars Based On Gravitational Correction

Neutron stars as one of the four astronomical discoveries in 1960 s, is famous for the super high temperature and density. Studies on neutron stars can be beneficial to understand the compact matter, get the interacting laws between compact matter and especially find the new matter forms. However, a few decades later, it has been no significative evolutions in the study on neutron stars. Now there are still a lot of things unknown about the matter, the structure and the cooling properties of neutron stars. With the progress in astronomical observations, gravitational corrections have been noticed and accepted by people. Especially, the gravitational correction is quite essential in neutron stars because of their high density. Therefore, influences of the gravitational correction on neutron star structures and cooling are studied here.The relativistic mean field theory(RMFT) and the relevant weak cooling theories are adopted to study the structures and cooling of neutron stars, and U bosons are introduced to describe the gravitational correction. Two kinds of neutron star matter are considered, one is the normal neutron star matter(containing protons, neutrons, electrons and muons), the other is the matter further containing ?? and 0? particles(0???np matter). There are five parts here: the progress in astronomical observations, including the mass, the gravitational redshift and the rotating of neutron stars are introduced in Part One; the basic theories, including RMFT, cooling theories in weak interaction, Tolman-Oppenheimer-Volkoff(TOV) equations and so on are given in detail in Part Two; influences of U bosons on the neutron star structures are studied in Part Three, and the relations between couple strength of U bosons and equation of state(EoS) and so on are described; effects of couple strength of U bosons on the neutrino emission from neutron stars and the regions where direct URCA process of nucleons(dURCA process) is allowed in neutron stars are investigated in Part Four; influences of gravitational correction on the cooling properties of neutron stars are studied in Part Five, and the behaviours of neutrino luminosity and cooling curves of the star with the inclusion of gravitational correction are also investigated. At last, conclusions and expectations are given.