Neutron stars are excellent laboratories to study the physics of matter at extreme conditions, which are beyond the scope of any terrestrial experiments. Recent multimessenger observations of neutron stars such as the measurements of the tidal deformability from the gravitational wave observation, the simulataneous mass and radius measurements of several pulsars in X-rays by the...
X-ray eclipse mapping is a valuable modelling technique capable of constraining the mass and radius of compact objects in eclipsing binaries and probing the outflow from the companion star. In this talk, I will demonstrate the capabilities and recent developments of the X-ray Transit and EClipse software, X-TREC, through the modelling of the X-ray eclipses observed in three systems: the...
The Equation of State (EoS) of ultra-dense matter inside Neutron Stars (NS) is one of the long-standing questions of modern astrophysics and a key science goal of NewAthena. To constrain the composition of this dense matter, we measure the macroscopic observables of NSs, such as their masses and radii. The most precise method to measure the radius of NSs is Pulse Profile Modeling (PPM), where...
Neutron stars (NSs) in quiescent low-mass X-ray binaries (qLMXBs) have been used in the past two decades for mass and radius measurements to better constrain the equation-of-state of dense matter. However, various sources of systematic uncertainties were put forward, possibly biasing the radius values by as much as 50%. They include the unknown NS spin and atmospheric composition, as well as...
In this contribution, I will start with an overview of different types of equation of state modelling in the Bayesian formalism, to demonstrate the িmpact of different experimental and observational constraints. Further, I will present equations of state at finite temperature obtained with Brussels-Skyrme-on-a-Grid (BSkG) energy density functionals developed at Brussels, which are unified...
