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2020

On the minimum radius of very massive neutron stars

Han, Sophia, Prakash, Madappa

Understand

Prospects of establishing the radii of massive neutron stars in PSR J1614-2230 and PSR J0740+6620 from NICER and Chandra observatories hold the potential to constrain the equation of state (EoS) of matter to densities well beyond those encountered in canonical stars of mass $\sim 1.4\,{\rm M}_{\odot}$.

In this work, we investigate the relation between the radii of very massive neutron stars up to the maximum mass, $M_{\rm max}$, supported by dense matter EoSs.
Results from models with hadronic matter are contrasted with those that include a first-order hadron-to-quark phase transition.
We find that a lower bound on $M_{\rm max}$ with an upper bound on the radius of massive pulsars serves to rule out too soft quark matter, and an upper bound on $M_{\rm max}$ with a lower bound on the radius of massive pulsars strongly disfavors a transition into too-stiff quark matter appearing at low densities.