From 36 neutron-star X-ray binaries, the best-fitting natal kick model is a bimodal Maxwellian with sigma=320 km/s for core-collapse supernovae and sigma=80 km/s for electron-capture supernovae.
Neutron Stars and Black Holes in X-Ray Binaries
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abstract
Galactic accretion driven stellar X-ray sources can be divided into groups in different ways. An important division, which covers almost all known X-ray binaries, can be made according to the mass of the donor star: high-mass X-ray binaries and low-mass X-ray binaries. Another distinction (partially overlapping with the previous one) can be made on the basis of the nature of the accreting object: a strongly magnetized neutron star, a neutron star with a weak magnetic field, or a black hole. In this review I describe the properties of these different types of X-ray binaries, and discuss the mass determinations which are the basis for distinguishing accreting neutron stars from black holes.
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On Neutron Star Natal Kicks in High-Mass X-Ray Binaries: Insights from Population Synthesis
From 36 neutron-star X-ray binaries, the best-fitting natal kick model is a bimodal Maxwellian with sigma=320 km/s for core-collapse supernovae and sigma=80 km/s for electron-capture supernovae.