We study the thermal structure of neutron stars with magnetized envelopes composed of accreted material, using updated thermal conductivities of plasmas in quantizing magnetic fields, as well as equation of state and radiative opacities for partially ionized hydrogen in strong magnetic fields. The relation between the internal and local surface temperatures is calculated and fitted by an analyt...

In the application of a micro-/nano-mechanical resonator, the position of an accreted particle and the resonant frequencies are measured by two different physical systems. Detecting the particle position sometimes can be extremely difficult or even impossible, especially when the particle is as small as an atom or a molecule. Using the resonant frequencies to determine the mass and position of ...

Context. Neutron stars in low-mass binary systems are subject to accretion when material originating from the companion star accumulates on surface. In most cases, justified and common assumption studying properties of neutron crust is fully accreted approximation. However, observations some X-ray transient sources indicate that original has not been completely replaced by material, but partly ...

The relationships between the effective surface (Teff ) and internal temperatures of neutron stars (NSs) with and without accreted envelopes are calculated for Teff > 5 × 104 K using new data on the equation of state and opacities in the outer NS layers. We examine various models of accreted layers (H, He, C, O shells produced by nuclear transformations in accreted matter). We employ new Opacit...

Many of the Milky Way's globular clusters are likely accreted from satellite galaxies that have long since merged with Way. When these susceptible to tidal disruption, this process starts already inside parent leading an early stellar stream within satellite. merges Way, cluster and its pre-merger in a somewhat chaotic process. Here, we investigate properties after merger as would see it today ...

We examine galaxy formation in a cosmological adaptive mesh refinement simulation, which includes two high-resolution boxes, one centred on a 3 × 1014 M cluster, and one centred on a void. We examine the evolution of 611 massive (M∗ > 1010 M ) galaxies. We find that the fraction of the final stellar mass which is accreted from other galaxies is between 15 and 40 per cent and increases with stel...

The accretion of hydrogen-rich matter onto C/O and O/Ne white dwarfs in binary systems leads to unstable thermonuclear ignition of the accreted envelope, triggering a convective thermonuclear runaway and a subsequent classical, recurrent, or symbiotic nova. Prompted by uncertainties in the composition at the base of the accreted envelope at the onset of convection, as well as the range of abund...

When a white dwarf (WD) is weakly magnetized and its accretion disk is thin, accreted material first reaches the WD’s surface at its equator. This matter slows its orbit as it comes into corotation with the WD, dissipating kinetic energy into thermal energy and creating a hot band of freshly accreted material around the equator. Radiating in the extreme-ultraviolet and soft X-ray, this material...

The stellar halos of galaxies encode their accretion histories. In particular, the median metallicity of a halo is determined primarily by the mass of the most massive accreted object. We use hydrodynamical cosmological simulations from the APOSTLE project to study the connection between the stellar mass, the metallicity distribution, and the stellar age distribution of a halo and the identity ...