The cooling phase of thermonuclear (type-I) X-ray bursts can be used to constrain neutron
star (NS) compactness by comparing the observed cooling tracks of bursts to accurate …

Determining neutron star (NS) radii and masses can help to understand the properties of
matter at supra-nuclear densities. Thermal emission during thermonuclear X-ray bursts from …

Thermal emission during X-ray bursts is a powerful tool for determining neutron star (NS)
masses and radii if the Eddington flux and the apparent radius in the cooling tail can be …

Observations of thermonuclear X-ray bursts from accreting neutron stars (NSs) in low-mass
X-ray binary systems can be used to constrain NS masses and radii. Most previous work of …

This paper presents a new analysis of the thermal emission from the neutron star (NS)
surface to constrain the dense matter equation of state. We employ an empirical …

Context. Relating different global neutron-star (NS) properties, such as tidal deformability
and radius, or mass and radius, requires an equation of state (EoS). Determining the NS …

We derive a new equation of state (EoS) for neutron stars (NS) from the outer crust to the
core based on modern microscopic calculations using the Argonne v 18 potential plus three …

A neutron star may cool much faster than through the'standard'scenario. Here we calculate
thermal evolution of neutron stars through various' nonstandard'fast cooling scenarios, and …

Cooling of neutron stars is calculated using an exact stellar evolution code. The full general
relativistic version of the stellar structure equations are solved, with the best physical input …

The masses and radii of low-magnetic field neutron stars can be measured by combining
different observable quantities obtained from their X-ray spectra during thermonuclear X-ray …