Population Synthesis of Old Neutron Stars in the Galaxy

Details Population Synthesis of Old Neutron Stars in the Galaxy Population Synthesis of Old Neutron Stars in the Galaxy

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000iaus..195..181p&link_type=abstract

Highly Energetic Physical Processes and Mechanisms for Emission from Astrophysical Plasmas, Proceedings of IAU Symposium #195, h

Statistics

Scientific paper

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 LE LE 550 km/s. 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, GT (or approximately) 200--300 km/s. The same conclusion is reached for both a constant (B ~1012 G) and an exponentially decaying magnetic field with a timescale ~109 yr. Present results, moreover, constrain the fraction of low-velocity stars which could have escaped pulsar statistics to < (or approximately) 1%.

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