The stages that follow the merging of two neutron stars are discussed. It is shown that if a rapidly rotating gravitationally bound object is formed after the merging (a spinar or a massive neutron star), then the characteristic time of its evolution is determined by a fundamental value tspin = 3k mpe 2h̄ mec 5/2G1/2 ≈ 10s · k, where the dimensionless value k = 100 ÷ 1000 depends on the exact eq...

In this poster I discuss the nature of the compact X-ray source in the center of the supernova remnant RCW 103. Several models, based on the accretion onto a compact object such as a neutron star or a black hole (isolated or binary), are analyzed. I show that it is more likely that the central X-ray source is an accreting neutron star than an accreting black hole. I also argue that models of a ...

X-ray observations suggest that neutron stars in low mass X-ray binaries (LMXB) are rotating with frequencies from 300 600 Hz. These spin rates are significantly less than the break-up rates for essentially all realistic neutron star equations of state, suggesting that some process may limit the spin frequencies of accreting neutron stars to this range. If the accretion induced spin up torque i...

Methods are developed for constructing spectral representations of cold (barotropic) neutron-star equations of state. These representations are faithful in the sense that every physical equation of state has a representation of this type and conversely every such representation satisfies the minimal thermodynamic stability criteria required of any physical equation of state. These spectral repr...

This paper gives an overview of the model of a neutron star with non-zero strangeness constructed within the framework of the nonlinear realization of the chiral SU(3)L x SU(3)R symmetry. The emphasis is put on the physical properties of the matter of a neutron star as well as on its internal structure. The obtained solution is particularly aimed at the problem of the construction of a theoreti...

Observations show that neutron stars can have space velocities much higher than those of their progenitors. On average pulsar birth velocities are in the range of 200-500 km/s and significant fraction might move with more than 1000 km/s (see [1] and references therein). The powerful and highly variable acceleration mechanism that leads to the measured velocities is still unclear. It is possible...

We discuss pycnonuclear burning of highly exotic atomic nuclei in deep crusts of neutron stars, at densities up to 10 g cm. As an application, we consider pycnonuclear burning of matter accreted on a neutron star in a soft X-ray transient (SXT, a compact binary containing a neutron star and a lowmass companion). The energy released in this burning, while the matter sinks into the stellar crust ...

We present limits to the log N − log S curve for isolated neutron stars, both cooling and accreting neutron stars, which are not active as radio pulsars, as observed with the ROSAT All-Sky Survey and compare it with theoretical expectations. So far, only one isolated neutron star is identified optically among ROSAT sources, namely RXJ185635-3754 (Walter & Matthews 1997). Three more promising ca...

We discuss the formation and evolution of binaries which contain neutron stars or black holes. It is shown that in a stellar system which for 10 yr had star formation rate similar to the current one in the Galactic disc, the rate of neutron star mergers is ∼ 2 × 10 yr, consistent with the observational estimates. The rate of black hole and neutron star mergers is by an order of magnitude lower....