Date:

Thu, 10/11/202213:00-14:00

Lecturer: Dima Ofegneim from the Hebrew University.

Abstract:

Neutron stars are known to be composed of extremely dense matter exceeding the density of atomic

nuclei for several times. Equation of state of this matter is still unknown in spite of a large number of

available theoretical models and the outstanding observational progress of the last few years. However,

some properties of neutron stars are almost insensitive to the equation of state model. Such

universalities are handful for studies of neutron stars. In the presented work, the existence of a tight

correlation between the mass, radius, central density, and pressure of maximum-mass neutron stars

modeled using diverse baryonic equations of state is demonstrated. A possible explanation for these

correlations is provided. Simple analytic forms of such correlations are suggested and compared with

observational constraints on the maximum mass of neutron stars and their radii. This gives a valuable

tool to constrain maximum pressure and density that could be reached in stable neutron stars, assuming

their equation of state is baryonic. Possible extensions and connections to other works are discussed.

Abstract:

Neutron stars are known to be composed of extremely dense matter exceeding the density of atomic

nuclei for several times. Equation of state of this matter is still unknown in spite of a large number of

available theoretical models and the outstanding observational progress of the last few years. However,

some properties of neutron stars are almost insensitive to the equation of state model. Such

universalities are handful for studies of neutron stars. In the presented work, the existence of a tight

correlation between the mass, radius, central density, and pressure of maximum-mass neutron stars

modeled using diverse baryonic equations of state is demonstrated. A possible explanation for these

correlations is provided. Simple analytic forms of such correlations are suggested and compared with

observational constraints on the maximum mass of neutron stars and their radii. This gives a valuable

tool to constrain maximum pressure and density that could be reached in stable neutron stars, assuming

their equation of state is baryonic. Possible extensions and connections to other works are discussed.