Constraints on the equation of state from the stability condition of neutron stars

Understand

The stellar equilibrium and collapse, including mainly white dwarfs, neutron stars and supper massive stars, is an interplay between general relativistic effects and the equation of state of nuclear matter.

• In the present work, we use the Chandrasekhar criterion of stellar instability by employing a large number of realistic equations of state (EoS) of neutron star matter.
• We mainly focus on the critical point of transition from stable to unstable configuration.
• This point corresponds to the maximum neutron star mass configuration.