Open AccessEvolution of neutron stars in high‐mass X‐ray binaries
Author(s) -
Urpin V.,
Konenkov D.,
Geppert U.
Publication year - 1998
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.1998.01771.x
Subject(s) - physics , neutron star , astrophysics , pulsar , accretion (finance) , roche lobe , x ray burster , x ray binary , astronomy , spin (aerodynamics) , binary star , stars , stellar evolution , stellar mass loss , thermodynamics
We consider the evolution of neutron stars during the X‐ray phase of high‐mass binaries. Calculations are performed assuming a crustal origin of the magnetic field. A strong wind from the companion can significantly influence the magnetic and spin behaviour of a neutron star even during the main‐sequence life of the companion. In the course of evolution, the neutron star passes through four evolutionary phases (‘isolated pulsar’, propeller, wind accretion, and Roche lobe overflow). The model considered can naturally account for the observed magnetic fields and spin periods of neutron stars, as well as the existence of pulsating and non‐pulsating X‐ray sources in high‐mass binaries. Calculations also predict the existence of a particular sort of high‐mass binary with a secondary that fills its Roche lobe and a neutron star that does not accrete the overflowing matter because of fast spin.