High-mass X-ray binaries (HMXBs) represent an important phase in the evolution of massive binary systems and provide fundamental information on the properties of the OB-star primaries and their compact secondaries (neutron star, black hole). Recent observations indicate that the neutron stars in some of these systems (Vela X-1, 4U 1700-37) are more massive than the canonical mass of 1.35 M . These observations have important consequences for the equation of state at supranuclear densities and the formation mechanism(s) of neutron stars and black holes: supernovae and gamma-ray bursts. As a consequence of the supernova explosion that produced the compact star in these systems, HMXBs have high space velocities and thus are runaways. Alternatively, OB-runaway stars can be ejected from a cluster through dynamical interactions Observations obtained with the Hipparcos satellite indicate that both scenarios are at work. © Copyright 2004: IA, UNAM.
CITATION STYLE
Kaper, L., Van der Meer, A., & Tijani, A. H. (2004). High-mass X-ray binaries and ob runaway stars. In Revista Mexicana de Astronomia y Astrofisica: Serie de Conferencias (Vol. 21, pp. 128–131). https://doi.org/10.1017/s0252921100008617
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