Abstract
The true nature and the internal constitution of the compact stars known as neutron stars (NSs) is one of the most fascinating enigma in modern astrophysics. We discuss some of the present models for the internal structure of NSs and the connection with the properties of ultra dense hadronic matter. In particular, we discuss the role of strangeness on the equation of state and the implications of the measurement of 2 solar mass NSs in PSR J1614-2230 and PSR J0348+0432.
Highlights
Neutron stars (NSs) are incomparable natural laboratories that allow us to investigate the fundamental constituents of matter and their interactions under extreme conditions that cannot be reproduced in terrestrial laboratories
One has to determine the equation of state (EoS) to extreme conditions of high density and high neutron-proton asymmetry, i.e. in a regime where the EoS is poorly constrained by nuclear data and experiments
As shown by various microscopic calculations [7,8,9,10] of the EoS of β-stable nuclear matter based on realistic nucleon-nucleon (NN) interactions supplemented with three-nucleon interactions (TNIs), it is possible to obtain NS sequences with maximum mass Mmax > 2 Msun and in agreement with presently measured masses
Summary
Neutron stars (NSs) are incomparable natural laboratories that allow us to investigate the fundamental constituents of matter and their interactions under extreme conditions that cannot be reproduced in terrestrial laboratories. As shown by various microscopic calculations [7,8,9,10] of the EoS of β-stable nuclear matter based on realistic nucleon-nucleon (NN) interactions supplemented with TNI, it is possible to obtain NS sequences with maximum mass Mmax > 2 Msun and in agreement with presently measured masses.
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