SIMBAD references

We show that mass accretion can explain the origin of pulsar glitches: a radial instability arises when a stable neutron star accretes matter, resulting in a partial or complete surface collapse. This is brought into relief by using the experimental data of pulsar PSR 1259-63, (the `rosetta pulsar'), whose existence proves that radiopulsars accrete matter. The conventional model of a radiopulsar consisting of a monolithic magnetic dipole field creating a light-cylinder mass accretion barrier is shown to be untenable. A more complicated model is discussed along the lines of a coronal pulsar model where small scale magnetic loops intersect neighboring neutron star platelets. Recent puzzling two-component ROSAT data of solitary radiopulsars is interpreted as a soft X-ray black-body thermal cooling spectrum and a mass accreted hard X-ray power-law tail. It is argued that the totality of the available X-ray emission data of pulsars indicates that most radiopulsars accrete matter and the high X-ray luminosity of PSR 1259-63 is due to its being able to accrete matter from a plentiful source of interstellar matter (its companion's stellar wind). Finally, we demonstrate that mass accretion can explain the unusual frequency of the big Vela pulsar glitches. An inescapable result of the analysis is the prediction that PSR 1259-63 will undergo a pulsar glitch (spin-up) in the near future due to the mass accretion of its companion's stellar wind.