TY - JOUR
T1 - A novel mechanism for creating double pulsars
AU - Sigurdsson, Steinn
AU - Hernquist, Lars
N1 - Copyright:
Copyright 2020 Elsevier B.V., All rights reserved.
PY - 1992/12/20
Y1 - 1992/12/20
N2 - Simulations of encounters between pairs of hard binaries, each containing a neutron star and a mainsequence star, reveal a new formation mechanism for double pulsars in dense cores of globular clusters. In many cases, the two normal stars are disrupted to form a common envelope around the pair of neutron stars, both of which will be spun up to become millisecond pulsars. We predict that a new class of pulsars, double millisecond pulsars, will be discovered in the cores of dense globular clusters. The genesis proceeds through a short-lived double-core common envelope phase, with the envelope ejected in a fast wind. It is possible that the progenitor may also undergo a double X-ray binary phase. Any circular, short-period double pulsar found in the galaxy would necessarily come from disrupted disk clusters, unlike Hulse-Taylor class pulsars or low-mass X-ray binaries which may be ejected from clusters or formed in the galaxy.
AB - Simulations of encounters between pairs of hard binaries, each containing a neutron star and a mainsequence star, reveal a new formation mechanism for double pulsars in dense cores of globular clusters. In many cases, the two normal stars are disrupted to form a common envelope around the pair of neutron stars, both of which will be spun up to become millisecond pulsars. We predict that a new class of pulsars, double millisecond pulsars, will be discovered in the cores of dense globular clusters. The genesis proceeds through a short-lived double-core common envelope phase, with the envelope ejected in a fast wind. It is possible that the progenitor may also undergo a double X-ray binary phase. Any circular, short-period double pulsar found in the galaxy would necessarily come from disrupted disk clusters, unlike Hulse-Taylor class pulsars or low-mass X-ray binaries which may be ejected from clusters or formed in the galaxy.
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U2 - 10.1086/186679
DO - 10.1086/186679
M3 - Article
AN - SCOPUS:11944270270
SN - 0004-637X
VL - 401
SP - L93-L96
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2 PART 2
ER -