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Evolution of high‐mass X‐ray binaries in the small magellanic cloud
Author(s) -
Yang J.,
Wik D. R.,
Zezas A.,
Laycock S. G. T.,
Hong J.,
Xu R.
Publication year - 2019
Publication title -
astronomische nachrichten
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.394
H-Index - 63
eISSN - 1521-3994
pISSN - 0004-6337
DOI - 10.1002/asna.201913557
Subject(s) - pulsar , physics , neutron star , astrophysics , x ray pulsar , astronomy , spin (aerodynamics) , binary pulsar , x ray binary , rotation (mathematics) , binary number , orbit (dynamics) , binary star , small magellanic cloud , stars , millisecond pulsar , geometry , mathematics , arithmetic , engineering , thermodynamics , aerospace engineering
To understand the progenitor of rotation‐powered pulsars, we compare them with accreting High‐Mass X‐ray binary pulsars, (hereafter X‐ray pulsars), in the small magellanic cloud. The diagram of spin period vs. period derivative shows that isolated neutron stars could be evolved from X‐ray pulsars. The pulsars with long spin period might spin up to 0.001–1 s. The binary orbit is disrupted by a third body in the universe, and the binaries are detached. Therefore, some of the pulsars become isolated neutron stars.