I propose a new type of common envelope jets supernova (CEJSN) events where instead single neutron star (NS; or black hole; BH) tight binary system NS and main sequence enters evolution (CEE) with red supergiant. The the merge inside supergiant enter CEE their own. accretes some mass through an accretion disk launches that explodes star. estimate two at this phase carry energy ~10^{52} erg, abo...

Since the discovery of first double neutron star (DNS) system, number these exotic binaries has reached fifteen. Here we investigate a channel DNS formation in binary systems with components above mass limit type II supernova explosion (SN II), i.e. 8 MSun. We apply spherically symmetric homologous envelope expansion model to account for loss, and follow dynamical evolution system numerically h...

We report the discovery during the Parkes Multibeam Pulsar Survey of PSR J1756−2251, a 28.5 ms pulsar in a relativistic binary system. Subsequent timing observations showed the pulsar to have an orbital period of 7.67 hrs and an eccentricity of 0.18. They also revealed a significant advance of periastron, 2.585± 0.002 deg. yr. Assuming this is entirely due to general relativity implies a total ...

this work focuses on modelling, optimal control and numerical simulation of the ship electric propulsion system provided by a double star synchronous machine. The in-depth analysis of the operation of the propulsion system of the vessel allowed us to model elements of the propulsion system. Thus, a non-linear global model was obtained describing the operation of the entire propulsion system. Th...

The glass transition in binary mixtures of star polymers is studied by mode coupling theory and extensive molecular dynamics computer simulations. In particular, we have explored vitrification in the parameter space of size asymmetry δ and concentration F2 of the small star polymers at fixed concentration of the large ones. Depending on the choice of parameters, three different glassy states ar...

We present optical spectroscopic observations of the massive X-ray binary LSI +65 • 010, the optical counterpart to the X-ray transient 2S0114+65. Our data show a dramatic variability in 1992 and only a mild variability during 1993–1995. An increase by a factor more than three in the equivalent width of the Hα emission line within four days is present in Nov. 1992. It is interesting to notice t...