We introduce a family of equations of state (EoS) for hybrid neutron star (NS) matter that is
obtained by a two-zone parabolic interpolation between a soft hadronic EoS at low densities …

We compute the tidal deformabilities for neutron star merger for equations of state with a
strong first order phase transition producing a new separate branch in the mass-radius …

We explore systematically a new class of two-phase equations of state (EoS) for hybrid stars
that is characterized by three main features: 1) stiffening of the nuclear EoS at …

We explore the connection between the stiffness of a hadronic equation of state (EoS) with a
sharp phase transition to quark matter to its tidal deformability. For this we employ a …

We demonstrate that future radius measurements of the NICER mission have the potential to
reveal the existence of a strong phase transition in dense neutron star matter by confirming …

We show that in the three-polytrope model of Hebeler et al.[Astrophys. J. 773, 11 (2013)
AJLEEY 0004-637X 10.1088/0004-637X/773/1/11] for the neutron star equation of state …

We investigate the implications of a hypothetical 2.5 M⊙ neutron star in regard to the
possibility of a first order phase transition to quark matter. We use equations of state (EoS) of …

Hadron-quark phase transition in neutron star cores is achieved in the present work with the
help of the Maxwell construction. For this purpose, we employ six different and well-known …

We explore the possible mass radius relation of compact stars for the equation of states with
a first order phase transition. The low density matter is described by a nuclear matter …

We examine which first order phase transitions are consistent with today's astrophysical
constraints. In particular, we explore how a well-constrained mass-radius data point would …