For neutron stars with hyperon-mixed core, neutrino emissivity is studied under the equation of state, obtained by introducing three-body force universal for all baryons so as to assure the maximum mass compatible with the observation. By paying attention to the density dependence of the critical temperatures of the baryon superfluids, which reflect the nature of baryon-baryon interaction and c...

1300nm edge-emitting multi-quantum-well lasers are the baseline choice for the optical transmitter in the CMS tracker optical links. The radiation environment is expected to be ~10Mrad and ~1014(neutron-equivalent)/cm2 over ten years. Lasers from four manufacturers have been irradiated in naked die form with neutron fluences of ~2x1014n/cm2. One laser type was also irradiated in a fully package...

We present spectroscopy and Hα imaging of a faint nebula surrounding the X-ray bright, nearby neutron star RX J1856.5−3754. The nebula shows no strong lines other than the Hydrogen Balmer lines and has a cometary-like morphology, with the apex being approximately 1′′ ahead of the neutron star, and the tail extending up to at least 25′′ behind it. We find that the current observations can be sat...

Recent calculations indicate that the cohesive energy of condensed matter increases with magnetic field strength and becomes very significant at magnetar-like fields (e.g., 10 keV at 3 × 10 G for zero-pressure condensed iron). This implies that for sufficiently strong magnetic fields and/or low temperatures, the neutron star surface may be in a condensed state with little gas or plasma above it...

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 · κ , where the dimensionless value κ = 100 ÷ 1000 depends on the exact e...

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 = κ m2pe 2h̄ mec 5/2G1/2 ≈ 7 · 10s · κ , where the dimensionless value κ depends on the exact equation o...

We study the ‘minimal’ cooling scenario of superfluid neutron stars with nucleon cores, where the direct Urca process is forbidden and enhanced cooling is produced by neutrino emission due to the Cooper pairing of neutrons. Extending our recent previous work, we include the effects of surface accreted envelopes of light elements. We employ the phenomenological density-dependent critical tempera...

In this paper we present a compilation of results from our most advanced neutron star merger simulations. Special aspects of these models were refered to in earlier publications (Ruffert & Janka 1999, Janka et al. 1999), but a description of the employed numerical procedures and a more complete overview over a large number of computed models are given here. The three-dimensional hydrodynamic si...

The origin of the local population of young, cooling neutron stars is investigated with a population synthesis model taking into account the contribution of neutron stars born in the Gould Belt, in addition to those originating in the Galactic disk. We estimate their emission in the soft X-ray band as a function of distance and age and construct the Log N – Log S distribution. It is shown that ...

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...