Neutron Rich Matter in Stellar Processes.

Prof.  Jirina Rikovska Stone

7月15号，星期三，下午2：00，物理馆103会议室

The microscopic composition and properties of stellar matter at a wide range of densities have been a subject of intense investigation for decades. In particular, compact objects such as hot proto-neutron and cold neutron stars have been in a for-front of interest. The scarcity of experimental and observational data has lead to the necessary reliance on theoretical models. Nuclear structure models play an important role in this effort as they provide an essential input to the equation of state, which is central to microscopic description of stellar objects.

I will survey the latest developments in construction of the Equation of State (EoS) of matter at zero and finite temperature assuming different mean-field models, including the non-relativistic Hartree-Fock + BCS Skyrme model relativistic mean field models. Predictions of Effective Density Functional, Quantum Monte Carlo and the Quark-Meson Coupling Model models for properties of neutron rich matter will be also shown.

Critical comparison of model EoS with available observational data on neutron stars, including gravitation mass, radii and cooling patterns and data on X-Ray burst sources and low mass X-ray binaries will be made.