The Neutron Star Census

The paucity of old isolated accreting neutron stars in ROSAT observations is used to derive a lower limit on the mean velocity of neutron stars at birth. The secular evolution of the population is simulated following the paths of a statistical sample of stars for different values of the initial kick velocity, drawn from an isotropic Gaussian distribution with mean velocity 0 ≤ V ≤ 550 km s −1. The spin–down, induced by dipole losses and the interaction with the ambient medium, is tracked together with the dynamical evolution in the Galactic potential, allowing for the determination of the fraction of stars which are, at present, in each of the four possible stages: Ejector, Propeller, Accretor, and Georotator. Taking from the ROSAT All Sky Survey an upper limit of ∼ 10 accreting neutron stars within ∼ 140 pc from the Sun, we infer a lower bound for the mean kick velocity, V ∼ > 200 − 300 km s −1 , corresponding to a velocity dispersion σ V ∼ > 125−190 km s −1. The same conclusion is reached for both a constant magnetic field (B ∼ 10 12 G) and a magnetic field decaying exponentially with a timescale ∼ 10 9 yr. Such high velocities are consistent with those derived from radio pulsar observations. Present results, moreover, constrain the fraction of low velocity stars, which could have escaped pulsar statistics, to less than 1%. Isolated neutron stars (NSs) are expected to be as many as 10 8 –10 9 , ∼ 1% of the total stellar content of the Galaxy. Young NSs, active as pulsars, comprise only a tiny fraction (∼ 10 −3 −10 −4) of the entire population , and about 1,000 have been detected in radio surveys. It is thus an observational fact that most of the NSs remain undetected as yet. Despite intensive searches at all wavelengths, only a few (putative) isolated NSs which are not radio pulsars (or soft γ repeaters) have been recently discovered in the X– All these sources emit a thermal spectrum at ≈ 100 eV and the derived column densities place them at relatively close distances (at most a few hundred parsecs) implying luminosities not in excess of 10 32 erg s −1. For RXJ1856-3754, an extremely faint optical counterpart (m V ∼ 26) have been firmly established by now (Walter & Matthews 1997) while a possible counterpart has been found …